CR propagation in our galaxy
I will present an overview of recent developments in numerical modelling of CR transport in our Galaxy. Corresponding numerical models aim at reproducing CR spectra and also diffuse gamma-ray emission from the Galaxy. For these numerical models we witness a transition from two-dimensional azimuthally symmetric models to those that use a more realistic description of our Galaxy. Focusing on results computed with the CR propagation code Picard, I will address the new physics that can be incorporated in such three-dimensional models. This includes, e.g., the impact of localised sources and also the possibility to investigate the effect of anisotropic diffusion with respect to the local magnetic field.